The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry

M. Bazot; M. J. Ireland; D. Huber; T. R. Bedding; A. M. Broomhall; T. L. Campante; H. Carfantan; W. J. Chaplin; Y. Elsworth; J. Meléndez; P. Petit; S. Théado; V. Van Grootel; T. Arentoft; M. Asplund; M. Castro; J. Christensen-Dalsgaard; J. D. Do Nascimento; B. Dintrans; X. Dumusque; H. Kjeldsen; H. A. McAlister; T. S. Metcalfe; M. J.P.F.G. Monteiro; N. C. Santos; S. Sousa; J. Sturmann; L. Sturmann; T. A. Ten Brummelaar; N. Turner; S. Vauclair

doi:10.1051/0004-6361/201015679

The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry

M. Bazot, M. J. Ireland, D. Huber, T. R. Bedding, A. M. Broomhall, T. L. Campante, H. Carfantan, W. J. Chaplin, Y. Elsworth, J. Meléndez, P. Petit, S. Théado, V. Van Grootel, T. Arentoft, M. Asplund, M. Castro, J. Christensen-Dalsgaard, J. D. Do Nascimento, B. Dintrans, X. DumusqueH. Kjeldsen, H. A. McAlister, T. S. Metcalfe, M. J.P.F.G. Monteiro, N. C. Santos, S. Sousa, J. Sturmann, L. Sturmann, T. A. Ten Brummelaar, N. Turner, S. Vauclair

Center for Space Science

Research output: Contribution to journal › Article › peer-review

Abstract

The growing interest in solar twins is motivated by the possibility of comparing them directly to the Sun. To carry on this kind of analysis, we need to know their physical characteristics with precision. Our first objective is to use asteroseismology and interferometry on the brightest of them: 18 Sco. We observed the star during 12 nights with HARPS for seismology and used the PAVO beam-combiner at CHARA for interferometry. An average large frequency separation 134.4 ± 0.3 μHz and angular and linear radiuses of 0.6759 ± 0.0062 mas and 1.010 ± 0.009 R⊙ were estimated. We used these values to derive the mass of the star, 1.02 ± 0.03 M⊙.

Original language	English (US)
Article number	L4
Journal	Astronomy and Astrophysics
Volume	526
Issue number	1
DOIs	https://doi.org/10.1051/0004-6361/201015679
State	Published - Dec 13 2010

Keywords

methods: data analysis
stars: individual: 18 Sco
stars: oscillations
techniques: interferometric
techniques: radial velocities

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1051/0004-6361/201015679

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Bazot, M., Ireland, M. J., Huber, D., Bedding, T. R., Broomhall, A. M., Campante, T. L., Carfantan, H., Chaplin, W. J., Elsworth, Y., Meléndez, J., Petit, P., Théado, S., Van Grootel, V., Arentoft, T., Asplund, M., Castro, M., Christensen-Dalsgaard, J., Do Nascimento, J. D., Dintrans, B., ... Vauclair, S. (2010). The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry. Astronomy and Astrophysics, 526(1), Article L4. https://doi.org/10.1051/0004-6361/201015679

Bazot, M, Ireland, MJ, Huber, D, Bedding, TR, Broomhall, AM, Campante, TL, Carfantan, H, Chaplin, WJ, Elsworth, Y, Meléndez, J, Petit, P, Théado, S, Van Grootel, V, Arentoft, T, Asplund, M, Castro, M, Christensen-Dalsgaard, J, Do Nascimento, JD, Dintrans, B, Dumusque, X, Kjeldsen, H, McAlister, HA, Metcalfe, TS, Monteiro, MJPFG, Santos, NC, Sousa, S, Sturmann, J, Sturmann, L, Ten Brummelaar, TA, Turner, N & Vauclair, S 2010, 'The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry', Astronomy and Astrophysics, vol. 526, no. 1, L4. https://doi.org/10.1051/0004-6361/201015679

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abstract = "The growing interest in solar twins is motivated by the possibility of comparing them directly to the Sun. To carry on this kind of analysis, we need to know their physical characteristics with precision. Our first objective is to use asteroseismology and interferometry on the brightest of them: 18 Sco. We observed the star during 12 nights with HARPS for seismology and used the PAVO beam-combiner at CHARA for interferometry. An average large frequency separation 134.4 ± 0.3 μHz and angular and linear radiuses of 0.6759 ± 0.0062 mas and 1.010 ± 0.009 R⊙ were estimated. We used these values to derive the mass of the star, 1.02 ± 0.03 M⊙.",

keywords = "methods: data analysis, stars: individual: 18 Sco, stars: oscillations, techniques: interferometric, techniques: radial velocities",

author = "M. Bazot and Ireland, {M. J.} and D. Huber and Bedding, {T. R.} and Broomhall, {A. M.} and Campante, {T. L.} and H. Carfantan and Chaplin, {W. J.} and Y. Elsworth and J. Mel{\'e}ndez and P. Petit and S. Th{\'e}ado and {Van Grootel}, V. and T. Arentoft and M. Asplund and M. Castro and J. Christensen-Dalsgaard and {Do Nascimento}, {J. D.} and B. Dintrans and X. Dumusque and H. Kjeldsen and McAlister, {H. A.} and Metcalfe, {T. S.} and Monteiro, {M. J.P.F.G.} and Santos, {N. C.} and S. Sousa and J. Sturmann and L. Sturmann and {Ten Brummelaar}, {T. A.} and N. Turner and S. Vauclair",

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T1 - The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry

AU - Bazot, M.

AU - Ireland, M. J.

AU - Huber, D.

AU - Bedding, T. R.

AU - Broomhall, A. M.

AU - Campante, T. L.

AU - Carfantan, H.

AU - Chaplin, W. J.

AU - Elsworth, Y.

AU - Meléndez, J.

AU - Petit, P.

AU - Théado, S.

AU - Van Grootel, V.

AU - Arentoft, T.

AU - Asplund, M.

AU - Castro, M.

AU - Christensen-Dalsgaard, J.

AU - Do Nascimento, J. D.

AU - Dintrans, B.

AU - Dumusque, X.

AU - Kjeldsen, H.

AU - McAlister, H. A.

AU - Metcalfe, T. S.

AU - Monteiro, M. J.P.F.G.

AU - Santos, N. C.

AU - Sousa, S.

AU - Sturmann, J.

AU - Sturmann, L.

AU - Ten Brummelaar, T. A.

AU - Turner, N.

AU - Vauclair, S.

PY - 2010/12/13

Y1 - 2010/12/13

N2 - The growing interest in solar twins is motivated by the possibility of comparing them directly to the Sun. To carry on this kind of analysis, we need to know their physical characteristics with precision. Our first objective is to use asteroseismology and interferometry on the brightest of them: 18 Sco. We observed the star during 12 nights with HARPS for seismology and used the PAVO beam-combiner at CHARA for interferometry. An average large frequency separation 134.4 ± 0.3 μHz and angular and linear radiuses of 0.6759 ± 0.0062 mas and 1.010 ± 0.009 R⊙ were estimated. We used these values to derive the mass of the star, 1.02 ± 0.03 M⊙.

AB - The growing interest in solar twins is motivated by the possibility of comparing them directly to the Sun. To carry on this kind of analysis, we need to know their physical characteristics with precision. Our first objective is to use asteroseismology and interferometry on the brightest of them: 18 Sco. We observed the star during 12 nights with HARPS for seismology and used the PAVO beam-combiner at CHARA for interferometry. An average large frequency separation 134.4 ± 0.3 μHz and angular and linear radiuses of 0.6759 ± 0.0062 mas and 1.010 ± 0.009 R⊙ were estimated. We used these values to derive the mass of the star, 1.02 ± 0.03 M⊙.

KW - methods: data analysis

KW - stars: individual: 18 Sco

KW - stars: oscillations

KW - techniques: interferometric

KW - techniques: radial velocities

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ER -

The radius and mass of the close solar twin 18 Scorpii derived from asteroseismology and interferometry

Abstract

Keywords

ASJC Scopus subject areas

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